「SPECTROSCOPIC」の共起表現一覧(1語右が「binary」)
該当件数 : 80件
This is a single-lined | spectroscopic binary system. |
3 Camelopardalis is a | spectroscopic binary in the constellation Camelopardalis |
It consists of a | spectroscopic binary and a third component. |
12 Camelopardalis is a | spectroscopic binary in the constellation Camelopardalis |
V373 Cas is a | spectroscopic binary in the constellation Cassiopeia. |
V357 Carinae (a Car, a Carinae) is a | spectroscopic binary in the constellation Carina. |
Theta-1 Sagittarii is a | spectroscopic binary lying 617 light years from Earth. |
θ1 Crucis (θ1 Cru, Theta1 Crucis) is a | spectroscopic binary star in the constellation Crux. |
The star e Serpentis (e Ser) is a | spectroscopic binary in the constellation of Serpens. |
It is a | spectroscopic binary whose components have an orbital pe |
It is a | spectroscopic binary whose components have an orbital pe |
It is a | spectroscopic binary with an orbital period of 143.6065 |
Pi Andromedae (π And, π Andromedae) is a | spectroscopic binary in the constellation Andromeda. |
It is a | spectroscopic binary and has a companion located 0.12 ar |
Secondary, Σ 1694 B is a | spectroscopic binary both A-type main sequence star. |
It is a | spectroscopic binary whose two components are separated |
104 Aqr A is a | spectroscopic binary and is suspected to be variable. |
VV Corvi (VV Crv) is a close | spectroscopic binary in the Corvus constellation. |
Lambda Andromedae is a | spectroscopic binary with an orbital period of 20.52 day |
It is a | spectroscopic binary with an orbital period of 134 days. |
θ2 Crucis (θ2 Cru / Theta2 Crucis) is a | spectroscopic binary star in the constellation Crux. |
This star is suspected of being a | spectroscopic binary, although this has not yet been con |
Theta Cephei is a white | spectroscopic binary star, located about 135 light-years |
First discovered | spectroscopic binary in 1889 by an American astronomer E |
Carl Vogel, Pickering discovered the first | spectroscopic binary stars. |
Alpha Equulei is a unique | spectroscopic binary star consisting of two components. |
Zeta Trianguli Australis (ζ TrA) is a | spectroscopic binary in the constellation Triangulum Aus |
It is a | spectroscopic binary whose components have magnitudes of |
Pi4 Orionis (π4 Ori, π4 Orionis) is a | spectroscopic binary star in the constellation Orion. |
The star has been found to be a | spectroscopic binary star. |
It is a | spectroscopic binary, whose components are separated by |
It is a | spectroscopic binary with a faint class-G companion. |
31 Camelopardalis is an eclipsing | spectroscopic binary in the constellation Camelopardalis |
de determination the orbital period of A's | spectroscopic binary difficult. |
A suspected | spectroscopic binary, it has now been resolved by speckl |
17 Leporis (17 Lep) is a | spectroscopic binary star in the constellation of Lepus. |
It is a suspected | spectroscopic binary, although this has not been confirm |
Beta Cephei is a triple star comprising a | spectroscopic binary with a magnitude 8 optical companio |
ilon Sagittarii (υ Sgr, υ Sagittarii) is a | spectroscopic binary star system in the constellation Sa |
The primary is a | spectroscopic binary, and its close companion completes |
Theta Aquilae is a | spectroscopic binary classified as a blue-white B-type g |
omponent, Iota Trianguli Australis A, is a | spectroscopic binary with a mean apparent magnitude of + |
(ε Her, ε Herculis) is a fourth-magnitude | spectroscopic binary star in the constellation Hercules. |
Iota Arietis is a | spectroscopic binary classified as a yellow G-type super |
of the system components, A and B, form a | spectroscopic binary that completes an orbit every 76 ye |
It is a | spectroscopic binary with components that are too close |
anis Majoris (ζ CMa, ζ Canis Majoris) is a | spectroscopic binary in the constellation Canis Major. |
Gliese 678 is a | spectroscopic binary star system approximately 60 light- |
This is a | spectroscopic binary, which means that the individual co |
HD 176051 is a | spectroscopic binary star system located approximately 4 |
It is also a | spectroscopic binary star with a period of almost 273 da |
This star is a | spectroscopic binary, and the primary is also a Beta Cep |
resolved Pismis 24-1SW and the unresolved | spectroscopic binary Pismis 24-1NE. |
In 1898 this system was reported to be a | spectroscopic binary system, with an orbital period of 2 |
omedae (Eta And, η Andromedae, η And) is a | spectroscopic binary star in the constellation of Androm |
Rho Tucanae is a | spectroscopic binary composed of two yellow-white F-type |
They are a | spectroscopic binary, meaning the separation between the |
Nu Andromedae is | spectroscopic binary whose components are a blue-white B |
It is a | spectroscopic binary, and the two subcomponents have app |
Chi Aurigae is a | spectroscopic binary which is classified as a blue-white |
The system consists of a | spectroscopic binary with a yellow G-type supergiant and |
rferometer was used to resolve a number of | spectroscopic binary systems, including Alpha Andromedae |
It is a | spectroscopic binary, which means it is a binary star wi |
Nu Scorpii A is itself a semi-detached | spectroscopic binary, having a fainter B-type companion |
name HR 2422 Monocerotis or HR 2422) is a | spectroscopic binary at a distance of around 6600 light- |
Kappa Velorum is | spectroscopic binary which is classified as a blue-white |
of the pair, Kappa Pegasi B, is actually a | spectroscopic binary, with the components designated Kap |
The star has also been identified as a | spectroscopic binary with a period of 494 days, but the |
Atik is a | spectroscopic binary star consisting of a spectral type |
It is a | spectroscopic binary having a 113.8 day period, indicati |
The orbit of a | spectroscopic binary is determined by making a long seri |
Kappa Arietis is a | spectroscopic binary which is classified as a white A-ty |
omedae was discovered to be a double-lined | spectroscopic binary in a series of spectra taken in 189 |
ae (V415 Car or A Carinae) is an eclipsing | spectroscopic binary of the Algol type in the constellat |
s (τ CMa, τ Canis Majoris) is an eclipsing | spectroscopic binary in the constellation Canis Major an |
l magnitude of approximately 5.15 and is a | spectroscopic binary star which consists of two giant st |
The system itself has been identified as a | spectroscopic binary star system; this means that Delta |
It is also a | spectroscopic binary, and is composed of two stars with |
At the centre of the system is a | spectroscopic binary, Iota Serpentis A and B. These are |
Tau Puppis is also a | spectroscopic binary star system in which the multiple c |
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